Euclid Science Capabilities - IN2P3 · PDF fileInstrument Overall WP Breakdown VG :5 Euclid WL...

Instrument Overall WP Breakdown VG :1

Euclid Consortium

Euclid Itzykson, IPhT-CEA Saclay June 18-20, 2012

Dark Energy with the

Euclid Space Mission

Y. Mellier On behalf of the Euclid

Consortium

http://www.euclid-ec.org

http://www.euclid-ec.org/




Euclid Consortium

Objective of the Euclid Mission



Euclid Consortium

• Understand the origin of the Universe’s accelerating expansion;

• Derive properties + nature of dark energy (DE), test gravity (MG)

• Distinguish DE, MG, DM effects…

• … Decisively by:

• using at least 2 independent but complementary probes

• tracking their observational signatures on the

• geometry of the Universe:

• Weak Lensing (WL), Galaxy Clustering (GC),

• cosmic history of structure formation:

• WL, Redshift-Space Distortion, Clusters of Galaxies

• controlling systematic residuals to a very high level of accuracy.

The ESA Euclid mission: scientific objectives



Euclid Consortium Distinguishing effect decisively

Parameterising our ignorance:

• DE equation of state: P/r = w and w(a) = wp + wa(ap-a)

• Growth rate of structure formation controlled by gravity: f ~ Wg , with g= 0.55 for general

relativity … if different, then GR not valid

1. Nature of the apparent acceleration

• Distinguish effects of L and dynamical dark energy Measure w(a) slices in redshift

• From Euclid data alone, get FoM=1/(Dwax Dwp) > 400:

if data consistent with L, and FoM > 400 then :

L favoured with odds of more than 100:1 = a “decisive” statistical evidence.

2. Effects of gravity on cosmological scales

• Probe growth of structure slices in redshift ,

• Separately constrain the metrics potentials (Y, F) as function of both scale and time

• Distinguish effects of GR from MG models with very high confidence level:

absolute 1-σ precision of 0.02 on the growth index, g, from Euclid data alone.

(1. + 2.) set the primary objectives of Euclid how can Euclid achieve this?



Euclid Consortium WL and GC: optimal primary probes for Euclid

• Weak Lensing (WL), wide field:

3-D cosmic shear measurements (tomography) over 0<z<2

probes distrib. of matter (D+L), expansion history, growth factor , Y+F.

shapes+distance of galaxies: shear amplitude, and bin the universe into

slices. For 0<z<2 photo-z sufficient, but with optical and NIR data.

• Galaxy Clustering (GC), wide field:

3-D position measurements over 0<z<2

probes clustering history of galaxies induced by gravity, Y , g, H(z).

3-D distribution of galaxies, but spectroscopic redshifts needed.

• GC and WL:

use the same survey (minimise complexity and cost)

use different data, complementary physical effects different systematics

• CG and WL are P(k,z) explorers:

both probe power spectra can be used also to probe dark matter (neutrino)

and inflation (non-Gaussianity and fNL)



Euclid Consortium

Cosmic Shear

survey

Galaxy Redshift

survey

Cosmological explorer

of gravity and fundamental physics

Dark Matter and Galaxy

Power Spectra with look back time

Other Euclid

probes

Legacy

Science (not discussed today)

VIS Imaging NIR Photometry NIR Spectroscopy

External

Photometry

External

Spectroscopy

Cosmo. Simul.

Planck, other

Space Euclid VIS and NIR observer of stars and galaxies

The Euclid Machine



Euclid Consortium The Euclid Mission: baseline and options

Shapes + Photo-z of n = 1.5 x109 galaxies ? z of n=5x107 galaxies

15,000 deg2

Ref: Euclid RB arXiv:1110.3193

40 deg2

Possibility to propose other surveys: SN and/or m-lens surveys, Milky Way ?

In ~5.5 years



Euclid Consortium Euclid:optimised for shape measurements

M51

SDSS @ z=0.1SDSS @ z=0.1 Euclid @ z=0.1Euclid @ z=0.1 Euclid @ z=0.7Euclid @ z=0.7

• Euclid images of z~1 galaxies: same resolution as SDSS images at z~0.05 and at

least 3 magnitudes deeper.

• Space imaging of Euclid will outperform any other surveys of weak lensing.


Euclid Consortium Third Euclid probe: Clusters of galaxies

• Clusters of galaxies: probe of peaks in density distribution

• number density of high mass, high redshift clusters very sensitive to

• any primordial non-Gaussianity and

• deviations from standard DE models

• Euclid data =

• 60,000 clusters with a S/N>3 between 0.2<z<2 (obtained for free).

• more than 104 of these will be at z>1.

• ~ 5000 giant gravitational arcs

very accurate masses for the whole sample of clusters (WL)

dark matter density profiles on scales >100 kpc

direct constraints on numerical simulations.

300000 strong galaxy lensing + 5000 giant arcs

test of CDM : probe substructure and small scale density profile.



Euclid Consortium Cluster with Euclid VIS+NIS imaging

Euclid combined

VIS+Y+J+H

images of a

simulated cluster


Euclid Consortium

Telescope and instruments



Euclid Consortium Main requirements to design the mission

Small PSF

Knowledge of the PSF size

Knowledge of distortion

Stability in time

External visible photometry for

photo-z accurary: 0.05x(1+z)

Catastrophic z < 10%

<z>/(1+z)<0.002

Understand selectionDeep field

• Completeness

• Purity

• WL and WL systematics

• GC and GC systematics

Wide survey Deep survey

Survey

size 15000 deg 2 40 deg2 N/S

VIS imaging

Depth ngal > 30/arcmin2

MAB =24.5 <z> ~0.9

MAB = 26.5

PSF size knowledge σ[R2]/R2<10-3

Multiplicative bias in shape

σ[m]<2x10-3

Additive bias in shape

σ[c]<5x10-4

Ellipticity RMS σ[e]<2x10-4

NIP photometry

Depth 24 MAB 26 MAB

NIS spectroscopy

Flux limit (erg/cm2/s)

3 10-16 5 10-17

Completness > 45 % >99%

Purity >80% >99%

Confusion 2 rotations >12 rotations



Euclid Consortium Current optical design

Telescope:

1.2 m Korsch , 3 mirror anastigmat, with a 0.45 deg. off-axis field , f=24.5m

Optically corrected and unvignetted FoV : 0.79 x1.16 deg2

VIS and NISP: share the same FoV (0.54 deg2)

Dichroic beam splitter at exit pupil : Visible and Near Infrared observations in parallel



Euclid Consortium Telescope and payload module

Telescope: 1.2 m Korsch , 3 mirror anastigmat, f=24.5m


Note: pointing error in spacecraft x,y direction

= 25mas over 600 s.

Reference: Laureijs et al 2012. SPIE.

FGS FPA = Fine Guidance Focal Plane Array:

mounted on the VIS FPA and part of the Attitude

and Control Orbit System (AOCS)

Payload block

diagram .

Typical telescope mechanical

architecture


Euclid Consortium VIS Instrument

Narrow band filters

(color gradient)

Suppressed .



Euclid Consortium NISP instrument

Camera Lens

Assembly (CaLA) Corrector Lens

Assembly (CoLA)

Calibration Unit (CU)

Structure Assembly (SA) & Thermal Control (TC) SiC

Temperature 140K

16 H2RG DETECTORS @ <100K+ ASIC

Sidecar@140K (provided by ESA/NASA)

• 16 NIR 2kx2k H2RG detectors

• 0.3 arc/pixel

• 4 Grisms (2 blue, 2 red, rotated

by 90 deg.) ;

• 3 NIR filters: Y, J H

• Telemetry= 180 Gbit/day

Filter Wheel Assembly (FWA)

Grism Wheel Assembly (GWA)


Euclid Consortium

Performances: • Survey,

• Images,and observables

• Cosmology



Euclid Consortium

• VIS and NISP observe in parallel

• 4x[(VIS+Grims)+(J,Y,H) then Grism change+dither]

• 4 different grism exposures

NISP+VIS field observing sequence

To Next Field



Euclid Consortium Optimal sky coverage for a fixed-length survey

• With 15,000 deg2 for for GC and WL: optimisation for a fixed time survey.

• Allows Euclid to do WL and GC simultaneously on the same area.

Consortium



Euclid Consortium Euclid Deep+Wide surveys feasible in 5.5 years

Euclid NAOJ June 6th 2012 14900 to 16100 deg2 in 5.5 years


Euclid Consortium NISP Performance: images/spectra/redshifts

All performances have been verified at image simulation level

True vs. measured redshift



Euclid Consortium VIS performance:imaging

A 4kx4k view of the

Euclid sky

VIS image: cuts made

to highlight artefacts

• Charge Transfer

Inefficiency (CTI) of CCDs

increases due to cosmic

rays.

Can be corrected to the

required level of accuracy.

• EC analysis: CTI has NO

impact on the P(k) and the

cosmology core program

Euclid IPMU June 1st 2012


Euclid Consortium

• Tomographic WL shear cross-power spectrum for

0.5 < z < 1.0 and 1.0 < z < 1.5 bins.

• Percentage difference [expected – measured]

power spectrum: recovered to 1% .

Input P(k)

B-modes

Euclid WL GC: DM and GC reconstructed P(k)



• Veff ≈ 19 h-3 Gpc3 ≈ 75x larger than SDSS

• Redshifts 0<z<2

• Percentage difference [expected – measured]

power spectrum: recovered to 1% .


Euclid Consortium Biasing and Growth rate

Optimistic = n gal density= 1.4 Red Book

Reference = n gal denstiy = Red Book (30/arcmin2)

Pesimisistic = n gal density = 0.5 Red Book

Amendola et al arXiv:1206.1225


Hu & Sawicki 2007

Amendola &

Quercellini 2003

Maartens & Majerotto 2006


Euclid Consortium

1-s, 2-s marginalised probability regions for constant g

and w

Reference = green regions

Optimistic = blue long-dashed ellipses

Pessimistic= black short-dashed ellipses

Euclid Cosmo predicted performances

g(z)= g0 + g1 [z/(1+z)]

1-s, 2-s marginalised probability regions for g0 and g1

Reference = yellow regions

Optimistic = green long-dashed ellipses

Pessimistic= black doted ellipses

Amendola et al arXiv:1206.1225



Euclid Consortium

DE constraints from Euclid: 68%

confidence contours in the (wp, wa).

Euclid combined: Cosmo predicted performances

Constraints on the g and ns.

Errors marginalised over all other

parameters.




Euclid Consortium Predicted FoM of the Euclid mission

Modified

Gravity Dark Matter

Initial

Conditions Dark Energy

Parameter g m n /eV fNL wp wa FoM

Euclid primary (WL+GC) 0.010 0.027 5.5 0.015 0.150 430

Euclid All 0.009 0.020 2.0 0.013 0.048 1540

Euclid+Planck 0.007 0.019 2.0 0.007 0.035 4020

Current (2009) 0.200 0.580 100 0.100 1.500 ~10

Improvement Factor 30 30 50 >10 >40 >400


More detailled forecasts given in Amendola et al arXiv:1206.1225



Euclid Consortium

Organisation, data

and

schedule



Euclid Consortium Euclid and Euclid Consortium organisations

EC:~950 members, 110 Labs

13 European countries • Austria, Denmark, France,

Finland, Germany, Italy,

Netherlands, Norway,

Portugal, Romania, Spain,

Switzerland, UK

+ Contributions from Berkeley

labs.

• Discussions: US/NASA ,

Canada/CSA, Belgium,

Sweden

EC contribution: ~1/3 of the

cost of the mission


Euclid

Consortium (EC)


Euclid Consortium Euclid/SGS flow and Organisation Units

• Total: ~ < 2PB of Euclid data (~ 106 images)

+ >10 PB of external data.

• Data volume for simulations may be much larger

• ESA Mission Operation Center

• ESA Science Operation Center

• Science Working Groups: 13 SWGs • Science objectives

• Requirements: pipeline products

• Requirements: pipeline performances

• Verify that the requirements are met

• Final science analyses

• Organisation Units: 10 OUs • Algorithmic definition of the processing

• Validating the implementation

OU scientists are from the SWGs

• Science Data Centers: 8 SDCs • Implementing pipelines

• Procuring local H/W and S/W resources

• SDC-DEV: algorithms robust codes

• SDC-PROD:integration on local

infrastructure, production runs of pipelines


Organisation Units EMA=Mission Archive


Euclid Consortium

• First release Level Q (Quick)

data release: 14 months after

the start of the survey (TBC)

•

• First complete data release:

26 months after the start of

the survey

• Then yearly releases

Data products and releases



Euclid Consortium

• October 4, 2011

• Spring 2012

• June 20, 2012 ?

• July 2012

• November 2012

• December 2012

• June 2013

• Q1 2014

• Q3/Q4 2017

• Q2 2020

• <(L+6 months)

• L+7 yrs

• L+9 yrs

Schedule

: Euclid selected as ESA M2 Cosmic Vision

: Completion of the Definition phase (A/B1)

: Adoption for the Implem. Phase (B2/C/D/E1)

: ITT release for PLM

: KO PLM contract

: ITT release for SVM

: KO SVM contract

: Instrument PDR

: Flight Model delivery

: Launch (L)

: Start Routine Phase

: End of Nominal Mission

: End of Active Archive Phase



Euclid Consortium Summary: Euclid

• ESA has selected the only space mission designed to

understand the origin of the accelerating universe;

• Put Europe at the forefront of one of the most fascinating

question of physics/cosmology of the next decades;

• Euclid will provide:

– tight constraints over the broadest range of DE; MG

models ever explored,

– unrivalled legacy value of VIS/NISP images and spectra;

• Extensive simulations have demonstrated it is feasible;

• Entering in implementation phase. Stay tuned until 2020…


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